Supernova shock breakout is an electromagnetic phenomenon in which observable features are highly sensitive to the motion and the shape of the shock front. Therefore it would be important to study the emission properties for obtaining information on the mechanisms of a stellar explosion and stellar evolution shortly before the explosion. The previous studies suggest that the shape of the observed light curve of XRO 080109/SN 2008D implies the asphericity of shock propagation (Suzuki & Shigeyama 2010a, Couch et al. 2011). Furthermore, the power-law feature of the observed X-ray spectrum can be reproduced by bulk-Compton scattering in the shock with a radial velocity of > 30% of the speed of light (Suzuki & Shigeyama 2010b). Though the studies have revealed the importance of the observational properties, there have been no studies which reproduce the shapes of the observed light curve and spectrum with a model, taking bulk-Compton scattering into account. In this study, we investigate the relationship between the properties of the emission and the motion of the shock, by using a toy model in which ejecta works as a piston in a spherically symmetric CSM. By using a Monte-Carlo method, we found that both the observed light curve and spectrum of XRO 080109 can be reproduced by a shock with a velocity of 60% of the speed of light and a circumstellar matter with a mass loss rate of 5.e-4 solar mass per year.

Supernova shock breakout is an electromagnetic phenomenon in which observable features are highly sensitive to the motion and the shape of the shock front. Therefore it would be important to study the emission properties for obtaining information on the mechanisms of a stellar explosion and stellar evolution shortly before the explosion. The previous studies suggest that the shape of the observed light curve of XRO 080109/SN 2008D implies the asphericity of shock propagation (Suzuki & Shigeyama 2010a, Couch et al. 2011). Furthermore, the power-law feature of the observed X-ray spectrum can be reproduced by bulk-Compton scattering in the shock with a radial velocity of > 30% of the speed of light (Suzuki & Shigeyama 2010b). Though the studies have revealed the importance of the observational properties, there have been no studies which reproduce the shapes of the observed light curve and spectrum with a model, taking bulk-Compton scattering into account. In this study, we investigate the relationship between the properties of the emission and the motion of the shock, by using a toy model in which ejecta works as a piston in a spherically symmetric CSM. By using a Monte-Carlo method, we found that both the observed light curve and spectrum of XRO 080109 can be reproduced by a shock with a velocity of 60% of the speed of light and a circumstellar matter with a mass loss rate of 5.e-4 solar mass per year.

The conventional particle interpretation of cold dark matter (CDM) still lacks laboratory support and struggles to explain the basic properties of dwarf galaxies. This tension motivates wave dark matter (ψDM) composed of extremely light bosons (m ψ ~10^(-22) eV), which suppresses structure below the kpc scale by the uncertainty principle but retains the large-scale structure predicted by CDM. In the first part of this talk, I will present the first cosmological ψDM simulations that achieve an unprecedented high resolution capable of resolving dwarf galaxies. These simulations reveal that every ψDM halo has a prominent soliton core surrounded by fluctuating density granules. These predictions compare favorably with the observations of galaxy formation, the Lyman-alpha forest and reionization, and also help explain gravitational lensing flux anomalies. The second part of the talk focuses on GAMER, a GPU-accelerated adaptive mesh refinement (AMR) code. A rich set of physics modules is incorporated and which outperforms other widely-adopted AMR codes by one to two orders of magnitude. The code scales well to thousands of GPUs and achieves a uniform resolution as high as 10,240^3 cells. I will present several ongoing astrophysical projects with GAMER that require substantially higher resolution than previously feasible, including turbulence cascade in galaxy cluster mergers, star formation in isolated disk galaxies, supermassive black hole accretion, and ψDM simulations.

18

2018-03-13 Tue14:20~15:20R1203

Kashiyama Kazumi[Tokyo U.]

Fast radio bursts and the young neutron star model

摘要

A growing number of fast radio bursts (FRB) has been detected but the source is still unknown. One of the leading models is the young neutron star model, in which a pulsar (or magnetar) of < 100 yrs-old surrounded by a wind nebula and supernova remnant are considered and connections between FRBs and luminous pulsar-driven supernovae are predicted. I will discuss multi-messenger/multi-wavelength approaches for testing the scenario.

19

2018-03-12 Mon11:00~12:00R1203

Andrew Cooper[University of Durham]

*專題研討*Galactic Archaeology: Simulations and Surveys

摘要

Many of the facilities poised to dominate optical and infra-red
astronomy over the next 20 years have put galactic archaeology (in a
nutshell, high-redshift science with low-redshift data) at the core of
their scientific programmes, including Gaia, PFS, HSC, LSST, MOONS,
JWST, WFIRST, ELT, MSE and TMT. They promise surveys of galactic
stellar halos, tidal streams and dwarf satellites with ultra-deep
photometry (exemplified by outstanding deep imaging from HSC) and
fine-grained spectroscopy of stars in the Local Group (the domain of
PFS). These data will provide stringent new probes of the evolving
relationship between star formation and the growth of cosmic structure
at the heart of the LCDM model, but only if we can successfully
combine Milky Way and extragalactic data in a sufficiently detailed
theoretical framework, integrated with results from other wavelengths
and epochs. In this talk I’ll outline my work to develop efficient
cosmological simulations (called STINGS) that bridge the gap between
all these exciting observations and the big picture questions of
galaxy formation theory. I’ll show quantitative insights these
simulations give into how the hierarchical disruption of satellites
contributes to galactic structure across scales ranging from the Milky
Way to the most massive clusters, and highlight some of the pressing
problems and priorities for this field. I’ll also give an update on
the DESI Milky Way Survey, an ambitious wide-area spectroscopy
programme targeting our own Galaxy’s stellar halo that will be highly
complementary to the Galactic Archaeology goals of PFS.

20

2018-03-07 Wed14:20~15:20R1203

Chiaki Hikage[Kavli IPMU]

Cosmology with Hyper-Suprime Cam cosmic shear analysis

摘要

The coherent pattern of distant galaxy images distorted by gravitational lensing of large-scale structure, i.e., cosmic shear, is a powerful probe of matter distributions in the Universe. Cosmic shear is a unique cosmological probe and is especially sensitive to the combination of the matter density parameter Ωm and the amplitude parameter of matter fluctuations σ8, i.e., S8(α) ≡ σ8(Ωm/0.3)^α with α ∼ 0.5. Recent cosmic shear measurements such as DES and KiDS prefers 2-3σ lower value of S8 than Planck CMB data in ΛCDM model. The tension may indicate some physics beyond ΛCDM model such as dynamical dark energy or modified gravity. Hyper-Suprime Cam (HSC) Subaru Strategic Program is a wide-field imaging surveys using a gigantic imaging camera on the 8.2-meter Subaru telescope. The unique property of the HSC is the combination of its depth (i~26 at 5σ) and excellent image quality (i-band seeing∼0.58”), which enables us to measure cosmic shear signals up to higher redshifts with lower shape noises than KiDS and DES. We measure cosmic shear power spectra with HSC survey first-year shear catalog covering 137 sq. deg. of the sky. The high effective number density of 16.5 per sq. arcmin after the photometric redshift cut of 0.3 ≤ z ≤ 1.5 allows a high significance measurement of cosmic shear signals with the total signal-to-noise ratio of 16 in the multipole range 300 ≤ l ≤ 1900. I present the current status of the HSC cosmic shear analysis.

21

2018-03-07 Wed11:00~12:00R1203

Kenneth Wong[NAOJ]

*專題研討*Studying the Dark Universe with Gravitational Lenses

摘要

Strong gravitational lensing is a powerful probe of the mass distribution in the Universe. Lensing is sensitive to the total mass distribution along the line of sight, making it a unique probe of dark matter in lensing galaxies, and useful for studying resolved properties of the magnified background sources. I briefly discuss applications of lensing magnification to recent ALMA observations of the lens SDP.9. Strong lensing is also valuable for cosmology through lensed quasars, which can be monitored to measure the "time delay" between the multiple images. This can be used to measure the "time-delay distance", which is primarily sensitive to the Hubble constant (H0). This method of measuring H0 is independent of type Ia supernovae and CMB observations, and may shed light on the growing H0 discrepancy between local universe and CMB measurements. I discuss the H0 Lenses In COSMOGRAIL’s Wellspring (H0LiCOW) project, which has measured H0 to ~3.8% precision for a flat Lambda CDM cosmology from three time-delay lenses. Our results are in moderate tension with the latest Planck results for a similar cosmology, hinting at possible new physics beyond the standard LCDM model and highlighting the importance of this independent probe. To improve this measurement, as well as leverage the power of strong lensing to study galaxy structure and magnified background sources, we require deep wide-area imaging surveys to build up a statistical sample of lenses, which are quite rare. The Hyper-Suprime Cam survey is an ongoing multiband imaging survey using the Subaru Telescope that will cover 1400 deg^2 of the sky to a depth of r~26. I present the current work of the HSC SSP strong lensing working group, which is focused on searching for new lenses and using these systems for studies of galaxy structure and cosmology. The search methods and science cases being developed now for surveys such as the HSC SSP are necessary to prepare for the upcoming revolution in strong lensing from LSST and Euclid, which will discover orders of magnitude more lenses than are currently known.

22

2018-03-05 Mon11:00~12:00R1203

Takashi Okamoto[Hokkaido University]

*專題研討*Simulations of galaxy formation --The roles of feedback

摘要

Cosmological hydrodynamic simulations are a powerful tool for studying non-linear formation processes of galaxies. Studies using cosmological galaxy formation simulations have revealed that "feedback", which is the process that gives energy and/or momentum to gas from stars and active galactic nuclei, plays crucial roles in galaxy formation. I explain how different feedback processes operate on different mass scales of galaxies. The simulations are also useful for observers as a tool to plan future observations. I briefly introduce how we collaborated with observers for ALMA observations of high-redshift emission line galaxies. Finally, I show some problems that current simulations have.

The driving and mass injection mechanisms of Active Galactic Nucleus jets are long-standing problems. M87 is the galaxy that has the second largest angular-size black hole and a relativistic jet, which allows us to test the theoretical models of these mechanisms. The edge brightened structure has been observed with VLBI in the downstream at least up to ~10^4 Rg from the black hole. This structure can be explained by the synchrotron emission from the steady axisymmetric electromagnetically-dominated jet (Takahashi et al. 2018). They reveal that the magnetic field lines must penetrate the black hole, not the accretion disk, and the black hole must rotate rapidly. Recent observations have shown a new feature, fork-like triple-ridge structure (Asada, Nakamura & Pu 2016; Hada 2017). We show that the above model with different electron density distributions can produce the triple-ridge structure. Such study will constrain the electron injection mechanism and will be required to improve the emission models around the black hole which would be observed by the Event Horizon Telescope.

24

2018-03-01 Thu14:20~15:20R1203

Guey-Lin Lin[NCTU]

Astrophysical neutrinos and new physics

摘要

Through many years of data taking, the IceCube observatory located at South Pole observed few tens of high energy astrophysical neutrinos. The flavor composition of these neutrinos could change during propagation as a result of neutrino oscillation and possible new flavor transition mechanism. Hence a precise measurement on the flavor composition of astrophysical neutrinos arriving on Earth could test new physics beyond Standard Model. In this talk, we shall review recent developments and future prospects of this research field.

25

2018-03-01 Thu11:00~12:00R1203

Ya-Wen Tang[ASIAA]

*專題研討*From filaments to circumstellar disks: on the star and planet formation at parsec and 100s AU scales

摘要

The details of what physical processes between turbulence, gravity, or magnetic field regulate the mass transfer from the large scales (several parsecs) of clouds and filaments onto the small scales of clumps and cores is still highly debated. The origin of such a debate resides in our (past) inability to track the magnetic (B) field properties over such a large range of scales and densities that are involved in the star formation process. In this talk, I will report the pioneer study of the correlation of the B field and velocity gradient, and the interplay between turbulence, gravity and B field within star forming filaments G34.43.
Different fragmentations within clumps are compared. For the second part of the talk, I will present the approaches to look for embedded planets within disks using the indirect evidences obtained from SUBARU, VLT, ALMA and future JWST.

26

2018-02-26 Mon11:00~12:00R1203

Hsi-Wei Yen[ESO]

*專題研討*Observational study of evolution from formation of protostellar disks to formation of planets

摘要

Protoplanetary disks, the sites of planet formation, are often observed around young stellar objects. However, it remains unclear as to how and when such disks form during the process of star formation, and whether they possess forming planets or not. Formation and evolution of disks are closely related to angular momentum transfer from their parental dense cores to the vicinity of protostars under the influence of the magnetic field. In this presentation, I will introduce my project aiming to link the analyses of the gas kinematics and the magnetic field in protostellar sources in order to understand the role of the magnetic field in disk formation and evolution. In addition, the gas kinematics in protoplanetary disks can exhibit signatures of dynamical interaction between planets and disks, and thus it can be a signpost of forming planets. In this presentation, I will also introduce my project of searching for planets embedded in protoplanetary disks by detecting signatures induced by disk-planet interaction.

27

2018-02-14 Wed14:20~15:20R1203

Paulo Freire[Max-Planck-Institut für Radioastronomie]

Discovery of five new, extreme double neutron star systems

摘要

Since the discovery of the first double neutron star system (also, the first binary pulsar), PSR B1913+16 (the famous Hulse-Taylor binary pulsar), such systems have been extremely valuable for tests of general relativity and the study of gravitational waves, decades before the LIGO detection. They have also been a great tool for studies of stellar evolution. In this talk I will present two of the most important systems known (the Hulse-Taylor and the ``Double Pulsar" system), but then emphasize the extraordinary systems discovered in the last 3 years, with a discussion of their enormous potential for advancing our knowledge of fundamental physics and stellar evolution. I then discuss some of the trends emerging from this study, particularly the correlation between the mass of the second-formed NS and the orbital eccentricity of the systems, and what this tells us about supernova astrophysics.

28

2018-02-13 Tue14:20~15:20R1203

Chi-Ting Chiang[Stony Brook University]

*專題研討*Simulating structure formation in different environments and the application

摘要

The observables of the large-scale structure such as galaxy number density generally depends on the density environment (of a few hundred Mpc). The dependence can traditionally be studied by performing gigantic cosmological N-body simulations and measuring the observables in different density environments. Alternatively, we perform the so-called "separate universe simulations", in which the effect of the environment is absorbed into the change of the cosmological parameters. For example, an overdense region is equivalent to a universe with positive curvature, hence the structure formation changes accordingly compared to the region without overdensity. In this talk, I will introduce the "separate universe mapping", and present how the power spectrum
and halo mass function change in different density environments, which are equivalent to the squeezed bispectrum and the halo bias, respectively. I will then discuss the extension of this approach to inclusion of additional fluids such as massive neutrinos. This allows us to probe the novel scale-dependence of halo bias and squeezed bispectrum caused by different evolutions of the background overdensities of cold dark matter and the additional fluid. Finally, I will present one application of the separate universe simulations to predict the squeezed bispectrum formed by small-scale Lyman-alpha forest power spectrum and large-scale lensing convergence, and compare with the measurement from BOSS Lyman-alpha forest and Planck lensing map.

29

2018-02-12 Mon14:20~15:20R1203

Yasuhiro Hasegawa[JPL]

*專題研討*Planet Formation in Star-Forming Regions: from the Solar System to Other Worlds

摘要

Planet formation is one of the fundamental ingredients in (exo)planetary sciences. Its importance is currently boosted up due to the recent significant progress of astronomical observations, theoretical modeling, and lab experiments. The most remarkable example may be the rapid accumulation of observed extrasolar planets and the characterization of their atmospheres. These studies are interesting in the sense that they can fill out a gap in research between the solar and extrasolar planetary systems. In this talk, I will present all the key results of my latest work. These include theoretical modeling of protoplanetary disks, out of which planetary systems are born, semi-analytical modeling of chondrule formation and the origin of asteroids, and a comprehensive analysis of solid accretion onto planets and its implications for the composition of observed exoplanets. In these studies, the outcome of the recent observations and lab experiments is utilized in order to derive new insights into the formation mechanisms of planets including the solar system. The combination of these attempts may enable us to move towards a comprehensive understanding of planet formation, covering a full size range from mm-sized, tiny dust grains to planetesimals and up to fully formed planets.

Stars are a fundamental unit of the universe, and their formation is a fundamental astrophysical process. The role of magnetic fields in star formation remains controversial today. I will discuss several molecular cloud and star formation theoretical ideas that have very different roles for magnetic fields and describe techniques for observing magnetic fields in regions of star formation. The talk will focus on the Zeeman effect, the only technique for directly observing magnetic field strengths. I will describe specific tests of vario Stars are a fundamental unit of the universe, and their formation is a fundamental astrophysical process. The role of magnetic fields in star formation remains controversial today. I will discuss several molecular cloud and star formation theoretical ideas that have very different roles for magnetic fields and describe techniques for observing magnetic fields in regions of star formation. The talk will focus on the Zeeman effect, the only technique for directly observing magnetic field strengths. I will describe specific tests of various theories of the role of magnetic fields in star formation and the application of observational results in those tests. Finally, I will describe briefly a star formation scenario that meets all of the observational tests, and mention future observational opportunities.
us theories of the role of magnetic fields in star formation and the application of observational results in those tests. Finally, I will describe briefly a star formation scenario that meets all of the observational tests, and mention future observational opportunities.

31

2018-02-01 Thu14:20~15:20R1203

Nanda Kumar[Universidade do Porto]

*專題研討*High-mass star formation: new observational insights

摘要

While the hunt for disks around high-mass stars continues in the ALMA era, other interesting predictions of high-mass star formation theories remain untested. Dense accretion flows leading to the formation of the highest mass stars can become Jeans unstable, producing a near-equal mass binary. This can explain the near-equal mass binarity well-known in field massive stars. I will show high-angular resolution observations (VLT and ALMA) of two such systems in formation. Young high-mass stars are also expected to be bloated, with radii up to 400Rsun, because of high internal entropy. I will present new infrared observations supporting this hypothesis. Finally, I will present a new systematic search and discovery of infrared variability in a large sample of young massive stars.

32

2018-01-31 Wed14:20~15:20R1203

James Wurster[Exeter]

￼The effect of non-ideal magnetohydrodynamics on star formation

摘要

Until recently, numerical simulations of low-mass star formation have been unable to produce large discs around a forming protostar. This contradicts observations. With the inclusion of non-ideal magnetohydrodynamics (MHD), large discs are now being formed in numerical simulations, indicating the necessity of non-ideal MHD. If the inclusion of non-ideal MHD can self-consistently re-introduce discs, then what effect will it have on the formation of the protostar itself, or on large scales in star forming clusters? In this talk, I will first introduce the three non-ideal MHD processes: Ohmic resistivity, ambipolar diffusion, and the Hall effect. I will then discuss their effects on disc formation, the formation and evolution of the first and second hydrostatic core, and (if time permits) on star cluster formation.

33

2018-01-23 Tue14:20~15:20R1203

Olivia Jones[University of Edinburgh]

Dust Production from Evolved Stars in the Local Group

摘要

Infrared observations of nearby galaxies and the Milky Way show that there are two main sources of ISM dust: the winds of evolved stars and supernovae ejecta. However, the total dust contribution from evolved stars relative to supernovae, and how it changes with metallicity, is less certain. Infrared photometric and spectroscopic Spitzer Surveys of the Large and Small Magellanic Clouds (LMC, SMC): Surveying the Agents of Galaxy Evolution (SAGE) resulted in the discovery of thousands of evolved stars. Here, I will describe how the composition and quantity of dust produced by these stars depends on metallicity. I will also discuss how the mid-IR stellar populations of the Magellanic Clouds can be used as a template for potential observations with JWST, and how we have applied this to our observing programs of Local Group galaxies and SN1987A with JWST.

34

2018-01-18 Thu14:20~15:20R1203

Haifeng Yang[University of Virginia]

*專題研討*Origins of (sub)millimeter disk polarization

摘要

Polarized (sub)millimeter emission from dust grains has long been established as a reliable way to probe magnetic fields in molecular clouds, based on the magnetic alignment of dust grains. At the same time, from theoretical studies, magnetic field is very important in the star formation and the evolution of protoplanetary disks, through either magnetorotational instability or magnetic-driven winds. The application of this method to the first resolved polarization observation in the protoplanetary disk HL Tau, however, yields rather unphysical magnetic field configuration and thus fails badly. This leaves an outstanding question: what are the origins of (sub)millimeter disk polarization? I will discuss the favored alternative mechanism, the “self-scattering” of dust grains, which successfully explains a lot of ALMA polarization observations to date. This brings both good news and bad news to the community. On the dark side, it’s harder to probe magnetic field with (sub)millimeter disk polarization, although we still found suggestive evidence in the IRAS 4A1 disk at long wavelength. On the bright side, polarization coming from “self-scattering” strongly depends on the properties of dust grains, including grain sizes, the optical depth, and thickness of dust disks. These allow us to study many important things, such as grain growth and dust settling.

35

2018-01-17 Wed14:20~15:20R1203

Andreas Schulze[NAOJ]

New constraints on the black hole spin in radio-loud quasars

摘要

One of the major unsolved questions on the understanding of the AGN population is the origin of the dichotomy between radio-quiet and radio-loud quasars. The most promising explanation is provided by the spin paradigm, which suggests radio-loud quasars to have higher black hole spin. However, the measurement of black hole spin remains extremely challenging.
We here present results comparing the mean radiative efficiencies of carefully matched samples of radio-loud and radio-quiet SDSS quasars at 0.3 1.5 in the radio-loud sample, suggesting that the radio-loud quasar population has on average higher black hole spin that the radio-quiet population. This provides observational support for the black hole spin paradigm.

36

2018-01-12 Fri14:20~15:20R1203

Somnath Dutta[S. N. Bose National Centre for Basic Sciences]

*專題研討*Stellar population and star formation histories of star-forming regions

摘要

The interaction between massive ionizing sources (O and early B-type) with their natal
molecular environment plays a constructive role of new generation star formation via. various
mechanisms e.g., Radiation Driven Implosion, collect & collapse process etc. The aim of this
colloquium is to understand some aspects of interaction of high and low mass stars with their
environment on the basis of observational evidences of massive ionizing sources, young stellar
contents and molecular/ionized gas properties. The young T Tauri stars show various types of
complex profiles on the infrared emission due to disk around them, strong emission lines on
their spectra, strong flux variation due to spot signatures. The characterization of those
phenomena could be directly addressed to the properties of these young stars, and also helps
to pick up the young population in a young cluster against the field population. Thus, multi-
wavelength studies of star-forming regions (SFRs) provide census of YSOs, their fundamental
parameters e.g. masses, ages, effective temperatures, circumstellar disks around them etc.
From such parameter space, broad pictures emerge on the young star-forming regions like star-
formation history, star-formation efficiency, timescales etc. We studied the stellar contents and
star formation activities of three distant Galactic SFRs (e.g. NGC 2282, Sh2-149 complex,
Cygnus OB7) using deep optical, near-Infrared, mid-Infrared and radio continuum observations.
We estimated the stellar content of NGC 2282, a young cluster in the Monoceros constellation,
using deep optical BVI and IPHAS photometry along with IR data from UKIDSS and Spitzer-
IRAC. With the aim of investigating star formation mechanism, we studied the Galactic H II
region Sh2-149 and associated molecular clouds with the help of optical spectra, CFHT-
WIRCAM, FCRAO 12CO(1-0), JCMT 13CO(3-2). Adiitionally, we performed CCD I-band time
series photometry of a young cluster NGC 2282 and Lynds 1003 cloud in Cygnus OB7 to
identify and characterize the variability of pre main-sequence stars.

In this talk, I aim to establish the important role played by ultra-strong magnetic fields to explain diverse astrophysical phenomena. First, I will talk about my doctoral thesis work on hypermagnetized white dwarfs. Such white dwarfs have strong interior magnetic fields greater than 4.4 x
10^{13} G, which introduce quantum mechanical effects, and also provide
additional pressure support against gravity, yielding highly
super-Chandrasekhar white dwarfs in the range 1.7-3.4 Msun. I arrived at
this conclusion by systematically progressing from a simple, spherically
symmetric, Newtonian model to a rigorous, non-spherical, general
relativistic model. Hypermagnetized white dwarfs have several important
astrophysical implications, the most compelling being their role as the
plausible progenitors of peculiar, highly over-luminous type Ia supernovae
(SNeIa). These SNeIa violate conventional Chandrasekhar-mass explosion
scenarios and seem to invoke white
dwarf progenitors having mass greater than 2 Msun. Finally, I will talk
about my current work on modeling the global properties of hypermagnetized
accretion disks. Local magnetohydrodynamic simulations of accretion flows
have shown that in the presence of a sufficiently strong but subthermal
(plasma-\beta = Pgas/Pmag > 1) vertical magnetic flux, a large-scale,
suprathermal toroidal field (plasma-\beta < 1) is generated, which becomes
the dominant source of pressure support in the disk. I term such
magnetically dominated disks as hypermagnetized accretion disks, which can
resolve several observational
shortcomings of the standard, geometrically thin, accretion disk model. I
have performed a global, linear stability analysis of hypermagnetized
accretion disks, whose results partly confirm the predictions of a local
model. However, it also reveals important differences that highlight the
necessity of a global treatment to accurately capture the geometric
curvature terms, which are otherwise neglected in weak-field studies of
accretion flows.

38

2018-01-10 Wed14:20~15:20R1203

Takaya Nozawa[NAOJ]

Consensus and issues on dust formation in supernovae

摘要

The role of core-collapse supernovae (SNe) as sources of cosmic dust
is the key to understanding the dust enrichment history in the universe.
Far-infrared and submillimeter observations with Herschel and ALMA
have revealed the presence of cool dust above 0.1 Msun in the ejecta
of SNe, which is in good agreement with masses of newly formed dust
predicted by theoretical studies. However, there remain two unsettled
issues: formation time and survivability of dust. Observationally, there
seems a growing pieces of evidence that dust mass gradually increases
with time over 20 years. However, we see from a simple argument that
this is not easy to be realized. On the other hand, the survivability of
dust against destruction by the reverse shock, which is critical to know
the final amount of dust ejection form SNe, is also hard to be evaluated
observationally. In particular, it depends on the initial size distribution
of dust, which is not constrained very well from infrared observations.
In this talk, I will introduce some recent approaches that address these
issues, and attempt to discuss how we can tackle them from now on.

39

2018-01-09 Tue14:20~15:20R1203

Tom Broadhurst[University of the Basque Country]

*專題研討*Fundamental Physics from the First Detections of Cosmological Neutrinos, Axions and Gravitational Waves

摘要

I will present the first direct evidence that the ubiquitous Dark Matter includes a small fraction of massive neutrinos (0.11eV summed over 3 flavours), with the rest composed of light axions (10^{-22}eV) in a Bose-Einstein state, motivated by String Theory. We have made the first cosmological simulations in this context, demonstrating the vast network of structure in the Universe is a beautiful interference pattern, with a standing solitonic wave at the center of every galaxy, representing the ground state. We have detected such a dark soliton in new detailed measurements of stars and gas at the center of our Galaxy.
Furthermore, the LIGO motivated "primordial black hole" interpretation of the Dark Matter is excluded by our new Hubble Space Telescope discovery of individual stars detected through the huge intervening columns of dark matter in galaxy clusters. Instead, these gravitational wave sources can be better interpreted as cosmologically distant, lower mass colliding black holes of stellar origin, that are lensed by intervening galaxies.